Computed spectral energy distributions of the IC cold pulsar wind emission, at periastron, for 11 different Γ_p, 0 values from Γ_p, 0 = 10 to 10⁵, for cases A (dotted lines), B (dashed lines), and C (solid lines) (cases B′ and C′ are very similar; see main text). A schematic spectral energy distribution based on the observed X-ray to gamma-ray emission around superior conjunction (adapted from Fig. 9 in Collmar & Zhang 2014; see references therein), which is close to periastron, is also shown.